activity
20242026
collaborators

8 papers

astro-ph.GA2026

The GALAH Survey: Neutron-Capture Elemental Abundances for 350,000 Gaia-RVS Spectra and the Chemodynamics of Accreted Structures

Pradosh Barun Das, Daniel B. Zucker, Aldo Mura-Guzmán +16

We present a comprehensive data-driven spectroscopic analysis of 357,415 red giant stars using Gaia DR3 Radial Velocity Spectrometer (RVS) spectra (8460-8700 A; ),…

astro-ph.EP2025

JWST NIRSpec finds no clear signs of an atmosphere on TOI-1685 b

Chloe E. Fisher, Matthew J. Hooton, Amélie Gressier +21

Determining the prevalence of atmospheres on terrestrial planets is a core objective in exoplanetary science. While M dwarf systems offer a promising opportunity, conclusive observ…

astro-ph.EP2025

Untapped: Veloce Detects Calcium in the Atmosphere of WASP-189b

Nicholas W. Borsato, Joachim Krüger, Daniel B. Zucker +3

High-resolution transmission spectroscopy has become a powerful tool for detecting atomic and ionic species in the atmospheres of ultra-hot Jupiters. In this study, we demonstrate…

astro-ph.EP2025

Atmospheric composition and circulation of the ultra-hot Jupiter WASP-121b with joint NIRPS, HARPS and CRIRES+ transit spectroscopy

Valentina Vaulato, Melissa J. Hobson, Romain Allart +57

Ultra-hot Jupiters like WASP-121b provide unique laboratories for studying atmospheric chemistry and dynamics under extreme irradiation. Constraining their composition and circulat…

astro-ph.GA2025

The GALAH Survey: Stellar parameters and abundances for 800,000 Gaia RVS spectra using GALAH DR4 and The Cannon

Pradosh Barun Das, Daniel B. Zucker, Gayandhi M. De Silva +15

Analysing stellar parameters and abundances from nearly one million Gaia Data Release 3 (DR3) Radial Velocity Spectrometer (RVS) spectra poses challenges due to the limited spectra…

astro-ph.EP2025

Titanium chemistry of WASP-121 b with ESPRESSO in 4-UT mode

B. Prinoth, J. V. Seidel, H. J. Hoeijmakers +15

Transit spectroscopy usually relies on the integration of one or several transits to achieve the S/N necessary to resolve spectral features. Consequently, high-S/N observations of…